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Investigation of Galilean Moons’ surface properties and atmospheric composition, temperature, and winds, and surface properties. This mode can also be used to characterize surface polarization by pointing 45◦off-nadir, after rotating the S/C by 90◦ around its nadir axis. It can also serve for solar occultation experiments to observe a weak molecular line in the atmosphere of Jupiter, a Galilean Moon, or the Europa torus. Flyby: Two CTS spectra are recorded for 30 seconds over 210 channels (16 bits coding). GCO: Two CTS spectra are recorded for 10 seconds over 130 channels (16 bits coding). In both cases, two CCH measurements (20 bits coding) are recorded for 0.1 sec, so that they are separated by maximum 1/2 beam at 1200 GHz. Solar occultation: Two CTS spectra are recorded for 60 seconds over 10000 channels (16 bits coding), and two CCH measurements (20 bits coding) are recorded for 0.1 second. Position-switch calibration method.




This mode will be used during phases I and III of the flybys, between −6hrs and −4.5hrs and between +3hrs and +4.5hrs from CA, and also continuously during phase II (from −1hr to +1hr of CA). During the whole GCO-500 phase, this mode will be used continuously for 5 orbits (i.e. 16-hrs) and then cycled equally with SWI_MOON_LIMB_SCAN_PS, SWI_MOON_LIMB_STARE_PS, and SWI_2D_MAP_PS. For polarization studies, this mode will be used much less often as it require a S/C rotation. Finally, it can be scheduled during solar occultations by Jupiter, moons, or the Europe torus.
any rule that is used to schedule the observation: repetition rules, continuous (plasma instruments), one-off, every orbit, every day, etc
conditions that make the observation not possible (e.g. thruster firing)